Since its construction in 1962, I have made solar observations monthly
at the McMath-Pierce facility on Kitt Peak. The main topics have been
magnetic fields (especially in sunspots), tracking the solar spectrum
observed in the sun-as-a-star and at disk center using the 13.5-m
spectrometer and the 1-m Fourier Transform Spectrometer, and the
making of spectrum atlases using the FTS.

SUNSPOT MAGNETISM
has been studied with the favorable Fe 15648A line
using an excellent dewer I inherited from Don Hall. With Sami Solanki
from ETH Zurich, spot regions were studied with polarization analysis.
Because polarization equipment is time consuming in setup, in recent
years we have simplified to total field measurements at the darkest
position in the spot umbrae. Because Fe 15648 is completely Zeeman
split in umbrae, such observations require no polarization equipment,
are independent of scattered light, and can readily be combined with
other spectral work. To date over 600 spots have been observed.

SUN-AS-A-STAR
synoptic observations. With Dick White at HAO, in Boulder,
we began tracking spectral irradiance of the sun in 1974 and continue
up to the present. Monthly observations are made with the grating
spectrometer; beginning in 1980 several records each year were collected
with the FTS. The solar 11 year cycle shows nicely in the Ca H & K,
H alpha, and Ca 8542 chromospheric lines. Temperature sensitive lines
around C 5380 have been studied by David Gray, revealing evidence of
long term secular change. For reasons that elude explanation, the FTS
archives failed to show the 1996 minimum in lines like Na D and
Mg b, and strong Fe. It is as if these lines, which are formed in the sun's
temperature minimum layer, are tracking a 22 year cycle. Also interesting
have been center disk measurements which indicate that the quiet solar
atmosphere is unaffected by the magnetic cycle.

SPECTRUM ATLASES (see sample)
have been compiled from FTS data. Lloyd Wallace is
the principal author. My role has been as an observer following Lloyd's
instructions. By making multiple observations at different air masses
it has been possible to separate the atmospheric and solar components.
Spectral coverage is 3570 to 220000A (28000 to 460cm-1) in the photosphere.
Complementary sunspot umbral atlases cover 4350 to 210000A (23000 to
470cm-1).

In the umbral atlases we recognize that the spectrum depends on the umbral
temperature, and so a range of spot conditions is presented. Solar line
identifications (atomic/molecular species) are made where practical. A
by-product was the discovery of water on the sun. As a service to the
science community hardcopies of the atlases were circulated by NSO
world-wide. Data is also posted on the internet; see below. A high
resolution poster of atmospheric absorbers, with identifications, has
also been published.